Constraints on Orbital Parameters from Secondary Eclipse Timing

Details Constraints on Orbital Parameters from Secondary Eclipse Timing Constraints on Orbital Parameters from Secondary Eclipse Timing

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.4205a&link_type=abstract

American Astronomical Society, DPS meeting #41, #42.05

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Scientific paper

The orbital phase of the midpoint of an extrasolar planet's secondary eclipse is determined solely by the orbital parameters eccentricity (e) and argument of periapsis (ω). Consequently, a precise measurement of the phase imposes a tight, but non-unique, constraint on these two parameters, which can be combined with other methods, such as radial velocity measurements, to estimate their values. By itself, the phase of secondary eclipse gives the value of the minimum eccentricity of the planet, providing strong evidence of whether the planet's orbit is circular or eccentric. We present orbital parameters derived from secondary eclipses of three different planets: Gliese 436 b, HAT-P-7 b, and HD 149026 b. These observations are part of the Spitzer Exoplanet Target of Opportunity program, which observes eclipses and transits of new exoplanets. Spitzer is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, which provided support for this work.

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